On the developmente of new viedeo stations to monitor meteorite-droppimg events over Spain

The SPanish Meteor and Fireball Network (SPMN) is an interdisciplinary project involving several universi- ties and research centres with the aim to study meteor and fireball events occurring over Spain and the bordering countries [1]. Large fireballs can be the precursors of meteorite falls and, so, the establishment of a network of detection systems is very con- venient in order to increase the chance of meteorite recovery by tracking their atmospheric trajectories and predicting the corre- sponding landing sites. To do this it is necessary to record the luminous trail from at least two different locations

Low-velocity cometary meteoroid streams encountering the earth: clues on the fragmentation of cometary aggregates and implications for interplanetary dust particles

Since 2005, the SPanish Fireball and Meteor Network (SPMN) is continuously monitor- ing meteor activity by using all-sky CCD and medium- field video cameras up to +3 to +4 meteor limiting magnitude [1,2]. One important goal of our network is the study of the meteoroid physico-chemical properties from multiple station data, together with meteor spec- tra. It is well known that the ablation behavior of me- teors in the Earth’s atmosphere shows photometric patterns that are reflecting important properties of the incoming meteoroids [3], but we are not yet fully un- derstanding such patterns. Besides, we are also trying to identify the main sources of large bolides to the Earth. As a consequence of the SPMN monitoring ef- fort, valuable trajectory and orbital data of meteors and fireballs is being obtained [4-6]. During 2007 several poorly-known meteoroid streams associated with com- ets were crossed by the Earth. We describe here unex- pected fireball activity, but focusing in low-velocity cometary streams. Particularly, we describe some me- teor outbursts and fireball events recorded by the SPMN during 2006-2007 that would be important de- livery sources of Interplanetary Dust Particles (IDPs). We try to encourage setting up future IDP campaigns for collecting cometary particles in the upper atmos- phere. By knowing the most important and favourable sources of cometary particles, and the dates of the en- counters with dense dust trails, such missions would be prepared in time for being successful

Robotic systems for meteor observing and lunar impact flashes detection in Spain

Since November 2008, a new robotic observatory is being setup by the University of Huelva within the environment of the Doñana Natural Park, in the south- west of Spain. Most of the systems in this astronomical observatory operate within the framework of the Spanish Meteor Network (SPMN), which is an interdisciplinary project dedicated to study meteoroids streams and the interaction of these particles of interplanetary matter with the Earth's atmosphere. For this we employ a system consisting of an array of high-sensitivity CCD video cameras for automatic meteor detection. Besides, an automated system for lunar impact flashes detection is being setup in collaboration with IAA-CSIC. This is based on three robotic telescopes that monitor the impact of meteoroids on the surface of the Moon. An important synergy is expected from the results recorded by both systems. Besides, climate conditions in this area provide us about 320 useful nights per year for astronomical observation, which makes this location ideal for this research project

A 2012 taurid bolide imaged in the framework of the Spanish fireball network

In 2010 the Spanish Meteor Net- work (SPMN) started a special program to obtain very precise orbital information on 2P/Encke meteoroids that is currently the focus of the author master thesis [1, 2]. The orbital similitude is a clear evidence on the connection between comets and meteor streams. The continuous sublimation of the ice-rich regions in cometary nuclei produces outgassing capable to re- lease cm to m-sized particles from cometary nuclei. This is the main way to produce meteoroid streams showers [3,4,5]. Another feasible physical process to produce cometary debris in heliocentric orbit is the disruption of a comet that explains the formation of about ten meteoroid streams [6,7,8]. This second pathway produces far larger particles that sometimes can even be in the meter scale and can explain very bright bolides associated with some meteor showers [8]. Unfortunately, large bolides are rare events so in order to study them a continuous sky monitoring is required which is the only way to collect information on the dynamic origin and physical behavior of large bolides penetrating Earth’s at mosphere. So far we have described different cases related to the Taurid complex [1,2]. Several Near Earth Objects (NEOs) have been dynamically associated w ith the Taurid complex clearly suggesting that the progressive disruption of a larger cometary progenitor is the source of this com- plex of bodies [9, 10]. In the current abstract we focus in a Taurid fireball named SPMN 201112 recorded on November 20 th , 2012 at 2h16m15.6s UT

A meteoroid from a Jupiter family comet recorded as a bright bolide in 2012

The continuous monitoring of meteor and fireball provides information about the origin and nature of meteoroids ablating in the Earth's atmosphere, but also about the mechanisms that deliver these materials to our planet. Thus, for instance, from the analysis of meteor events simultaneously imaged from, at least, two different locations it is possible to obtain atmospheric trajectories, radiant, orbital and physicochemical parameters such as the mass of the meteoroids and the tensile strengths of these particles [1, 2, 3]. In addition, meteor spectroscopy provides helpful information about the chemical nature of meteoroids [5, 6, 7]. With this aim, the SPanish Meteor Network (SPMN) is performing a continuous fireball monitoring and meteor spectroscopy campaign over Spain and neighbouring areas. Here we present orbital and chemical information derived from the analysis of a fireball imaged in 2012. This event was produced by a meteoroid from a Jupiter Family Comet

Spectra of bolides produced by meteoroids from (3200) phaeton

The Geminids is the densest annual meteoroid stream whose parent body is asteroid (3200) Phaethon, which was considered by some researchers as an extinct cometary nucleus rather than a regular asteroid [1]. On the basis of spectral and dynamical similarities, it has been recently proposed that asteroid 2 Pallas is the likely parent body of asteroid (3200) Phaeton [2, 3]. The asteroidal origin of the Geminids suggests that this stream could be a potential meteorite producer. The analysis of several Geminid fireballs observed between 2009 and 2010 from Spain supports this idea [4]. In this work we present the preliminary analysis of four emission spectra produced by meteoroids from the Geminids stream. These were obtained in the framework of the continuous spectroscopic campaign developed by the SPanish Meteor Network (SPMN)

On the chemical nature and orbit of meteoroids from the omicron draconid stream

The omicron Draconids were first observed by Denning in the 19th Century [1]. The activity was, however, modest, with a zenithal hourly rate (ZHR) of about 10–12. Denning [2] also reported observations in 1929 but in neither case was an orbit given, only a radiant position (RA ~271º, Dec. ~60º). However, for a considerable time after Denning’s observations, no records of any activity exist. Whether this is due to a lack of observers at the pertinent time (early July and thus close to the longest day and also close to the activity period of the delta Aquariids and observers may have preferred to study those) or an intrinsic lack of activity from the Omicron Draconids is not clear. The next record appears to be by Cook et al. [3] reporting on the work of the Harvard Meteor Project in the 1950s. In that paper they also suggested that the formation of the stream was associated with the disintegration of the nucleus of comet C/1919 Q2 Metcalf. In fact, our team recorded in 2008 a mag. -18 omicron Draconid fireball which was linked to this comet [4]. Here we present the analysis of a doublestation omicron-Draconid fireball recorded in the framework of our continuous fireball monitoring and spectroscopic campaigns in July 2007. The unique spectrum obtained for a member of this stream has provides helpful information about the chemical nature of meteoroids in the omicron-Draconid stream

The Northern χ -Orionid meteoroid stream and possible association with the potentially hazardous asteroid 2008XM1

We present new orbital data and dynamic results pointing towards the origin of the Northern χ -Orionid meteoroid stream, which is a part of the Taurid meteoroid complex. A new software package was developed to establish the potential parent bodies of meteoroid streams based on the similarity of their orbits. The analysis of a Northern χ -Orionid fireball observed on 2011 December 6 identified two potential parent bodies: the near-Earth object (NEO) 2002XM35 (previously proposed as the parent of this meteoroid stream) and the more recently discovered potentially hazardous asteroid 2008XM1. The calculation of the evolution of the orbital elements performed by using the Mercury 6 symplectic integrator supports the idea that 2008XM1 is a better parent body. Our data sample was expanded by including also in the calculations the mean orbit of the χ -Orionid stream. The results are consistent with the fragmentation of a larger body in the past that could give rise to both NEOs and the Northern χ -Orionid stream. To confirm this, further observations to improve the orbital elements of these asteroids should be attempted before the objects are lost. The analysis of the emission spectrum recorded for this fireball supports a primitive nature for these meteoroids.Ministerio de Ciencia e Innovación AYA2009-13227, AYA2009-14000-C03- 01, AYA2011-26522CSIC 201050I043Junta de Andalucía P09-FQM-455

A bright bolide produced by a meteoroid follwing a Jupiter family comet orbit

One of the techniques employed by the SPanish Meteor Network (SPMN) to monitor the night sky is based on high-sensitivity CCD video de- vices. These have a limiting magnitude of +3/+4 with- out using any image intensifier. Our meteor network has increased the number of such video stations from 2 in 2006 to 25 in 2011. Nowadays we perform a con- tinuous monitoring of meteor and fireball activity over Spain and neighbouring regions, which is equivalent to an area of about 500.000 km 2 . This expansion is being accompanied by a considerable effort to develop sev- eral software packages to accomplish different tasks, such as the automated operation of some of our sta- tions and the data reduction of the huge amount of information these provide. Besides, favourable weather conditions in Spain combined with the high sensitivity of our systems give us an advantage to per- form this continuous monitoring, which has provided important information about meteor and fireball activ- ity. The analysis of bolides is, in fact, one of our pri- orities, as brighter ones can be potential meteorite pro- ducing events and fireballs also may provide useful information about disruption episodes in their parent objects. In this context, we have imaged on April 27, 2011 a double-station sporadic fireball with an abso- lute magnitude of about -7 ± 1. The analysis of this bo- lide is made here

A northerm may ophiuchid fireball imaged in 2012 in the framework of the Spanish meteor network

The Northern May Ophiuchids is a poorly known annual meteor shower whose activity period extends from April, 25 to May, 31, peaking around May 13 [1]. It is included in the IAU list of working meteor showers with code 149 NOP. Thus, the development of a continuous observing campaign can provide helpful data to increase or knowledge about this shower. In particular, multi-station events would be useful to calculate precise orbital data and different physico-chemical properties of meteoroids belonging to the NOP stream. Besides, the chemical nature of these particles of interplanetary matter can be inferred from the analysis of the emission spectrum produced when they ablate in the atmosphere. Here we present the analysis of a NOP fireball recorded in the framework of the fireball monitoring and spectroscopic campaign organized by the SPanish Meteor Network (SPMN)